Difference between revisions of "LBNL-2020: Extragalactic Foreground Modeling"

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* Yuuki Omori - MultiDark
 
* Yuuki Omori - MultiDark
 
* Giuseppe Puglisi - [https://www.dropbox.com/s/gurkiivrtknkzfa/modeling_polfrac_S4_01_04_2020.pdf?dl=0 Modelling of polarized sources]
 
* Giuseppe Puglisi - [https://www.dropbox.com/s/gurkiivrtknkzfa/modeling_polfrac_S4_01_04_2020.pdf?dl=0 Modelling of polarized sources]
* Nikhel Gupta - Modelling of polarized Sources
+
* Nikhel Gupta - [https://stanford.box.com/s/yeeu5qtad8z5ld1d4sliuamsdv3zb1y0 Modelling of polarized Sources]
  
 
== Notes ==
 
== Notes ==
 
google slide link: https://docs.google.com/document/d/1S-Wo1p4yEj7AZQP1EqABbGyYU6OcRsjX-0acRaayAKw/edit
 
google slide link: https://docs.google.com/document/d/1S-Wo1p4yEj7AZQP1EqABbGyYU6OcRsjX-0acRaayAKw/edit

Revision as of 11:12, 1 April 2020

Charge

1. Within S4:

  a. Any developments since the last meeting in terms of                       
      code/implementation/methods/validation using existing data?
      Are there any external simulations that we could make use of?
  b. Identify the group and specific science that critically relies on simulations.
  c. Reassess the usage and requirements (number of realizations? resolution? Hydro?)  
      - Do the existing simulations satisfy the requirements? (e.g. accuracy at high-ell)
      - Have we tested that all the key measurements can be done on the simulations? 
  d. Which observables do we need to prioritize (Dust, Sync, AME, tSZ, latetime-kSZ, 
      patchy-kSZ,CIB,sources)? 

2. Communication with groups out of S4 (for cross-correlation studies)

  a. How do we set up an MOU?   
  b. How to set up a framework to implement each other’s pipelines? 


Agenda

Notes

google slide link: https://docs.google.com/document/d/1S-Wo1p4yEj7AZQP1EqABbGyYU6OcRsjX-0acRaayAKw/edit